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arxiv: 2606.18352 · v1 · pith:OE5UAP7Knew · submitted 2026-06-16 · 🌌 astro-ph.GA

TNG SAM: Bridging Hydrodynamical Complexity and Semi-Analytic Efficiency to Model Galaxy Formation

Osase Omoruyi , Bryan A. Terrazas , Yossi Oren , Austen Gabrielpillai , Viraj Pandya , Rachel S. Somerville , Amiel Sternberg , Lars E. Hernquist This is my paper

Pith reviewed 2026-06-26 23:38 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords galaxy formationsemi-analytic modelshydrodynamical simulationsbaryon cyclinggalaxy evolutionstellar feedbackmetal circulationcosmological modeling
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The pith

A calibrated semi-analytic model reproduces hydrodynamical galaxy and halo properties within 30 percent accuracy out to redshift 6.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This paper introduces updates to a semi-analytic model for galaxy formation, including new ways to handle halo gas re-accretion, cooling without a strict cold or hot mode split, explicit treatment of outflows at galactic and halo scales, star formation efficiency, and the movement of metals. These updates are calibrated so that the model matches the flow of gas and metals as well as overall galaxy and halo properties from hydrodynamical simulations in a specific mass range. The match holds to within roughly 30 percent out to redshift 6. A sympathetic reader cares because this provides an efficient way to model galaxy evolution over the large volumes that future surveys will observe, something full hydrodynamical simulations struggle to do at scale.

Core claim

With updates to halo gas re-accretion efficiency, a cooling model that goes beyond the traditional cold or hot mode split, explicit galactic and halo outflows, star formation efficiency, and metal circulation between galaxies and surroundings, the model reproduces the gas and metal flows from galaxy to halo scales as well as global properties within 30 percent accuracy out to redshift 6 after calibration on stellar feedback dominated galaxies.

What carries the argument

The updated semi-analytic model that incorporates targeted changes to gas cycling and feedback processes to align with hydrodynamical simulation results.

If this is right

  • Such a model enables study of galaxy evolution across large cosmological volumes needed for future observational surveys.
  • The complex physics of gas and metal flows in galaxy formation can be captured in an efficient analytic framework.
  • Global properties of galaxies and halos are matched to within 30 percent accuracy across a range of redshifts.
  • The approach bridges the detail of hydrodynamical simulations with the speed of semi-analytic methods.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Rapid parameter variation studies become possible that would be too costly in full hydrodynamical simulations.
  • Calibration to a broader range of halo masses could extend the model's reach to different galaxy populations.
  • Direct comparisons with wide-field survey data could become more feasible with this efficient modeling tool.

Load-bearing premise

The calibration performed only on stellar feedback-dominated galaxies in halos from about 10 billion to 1 trillion solar masses captures the key baryon cycling physics needed for accuracy at all redshifts and for all galaxy properties.

What would settle it

A comparison where the model's predicted stellar masses or hot halo gas masses deviate by more than 30 percent from those in the hydrodynamical simulation at redshifts or masses outside the calibration sample would disprove the central claim.

Figures

Figures reproduced from arXiv: 2606.18352 by Amiel Sternberg, Austen Gabrielpillai, Bryan A. Terrazas, Lars E. Hernquist, Osase Omoruyi, Rachel S. Somerville, Viraj Pandya, Yossi Oren.

Figure 1
Figure 1. Figure 1: A sample Mhalo∼ 1011.3M⊙ central subhalo (ID: 609911) from TNG100 is shown to illustrate how TNG’s out￾puts are compared to the SAM. The map is color-coded by total gas mass, with brighter regions indicating higher mass concentrations. In TNG, we define the interstellar medium (ISM) as all material within twice the stellar half-mass radius (solid blue circle), and the circumgalactic medium (CGM) as all mat… view at source ↗
Figure 2
Figure 2. Figure 2: Comparison of global galaxy-scale properties (panels i.–iv.) and flow rates (panels v.–ix.) between TNG100 (dotted lines) and the Santa Cruz SAM (dashed squares). Each panel shows median trends as a function of halo mass, color-coded by a representative subset of redshifts (z = 0, 1, 2, 4, 6): darker colors correspond to lower redshift and lighter colors to higher redshift, ranging from dark purple to yell… view at source ↗
Figure 3
Figure 3. Figure 3: As in [PITH_FULL_IMAGE:figures/full_fig_p012_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Illustration of the TNG SAM, calibrated to reproduce the baryon cycle of central galaxies in the TNG100 simula￾tion. The diagram shows the main baryonic reservoirs—cold gas (Mcold), stars (Mstar), hot halo gas (Mhot), and ejected gas (Mejected)—and the flows of gas and metals between them. Arrows represent baryon flow directions, with governing parameters labeled in purple (e.g., tcool regulates cooling fr… view at source ↗
Figure 5
Figure 5. Figure 5: Overview of the scaling relations measured from TNG100 and the subset of TNG100 galaxies analyzed by YO25, organized by relations regulating gas flows, star formation, and metal flows. Each panel shows the distribution of TNG100 values as a function of halo mass and over redshift as dotted lines colored by redshift. Solid lines show analytic fits based on the well-resolved sample (100-400 galaxies per reds… view at source ↗
Figure 6
Figure 6. Figure 6: Functions that govern the TNG SAM’s stellar feedback-driven outflows at the scale of the galaxy (left and middle panels) and halo (right panel) across redshift. The left panel shows that the mass loading factor ηISM (solid lines), defined as the ratio of the outflow rate to the star formation rate, almost always exceeds the launch value from star-forming gas cells in TNG (dotted lines), suggesting addition… view at source ↗
Figure 7
Figure 7. Figure 7: Comparison of halo-scale quantities (panels i–ii.) and the corresponding gas and metal flow rates (panels iii–vi.) between TNG100 (dotted lines) and the newly calibrated TNG SAM (dashed triangles). The TNG SAM reproduces the hot gas mass and hot gas metallicity within ±30% across most halo masses and redshifts. Gas and metal inflow rates are similarly well-matched, typically within ±30% of TNG. A major imp… view at source ↗
Figure 8
Figure 8. Figure 8: Comparison of galaxy-scale properties (panels i–v.) and flow rates (panels vi–ix.) between TNG100 (dotted lines) and the newly calibrated TNG SAM (dashed triangles). As in [PITH_FULL_IMAGE:figures/full_fig_p020_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: To show the importance of each modification made to the TNG SAM, we illustrate how reverting individual model components to their original SC SAM formulations impacts the TNG SAM’s ability to reproduce TNG’s global results at the galaxy and halo scales at z = 0. The solid black line represents the 50th percentile of the fully calibrated TNG SAM, while the shaded gray region marks ±30% of the TNG100 populat… view at source ↗
Figure 10
Figure 10. Figure 10: Continuation of [PITH_FULL_IMAGE:figures/full_fig_p022_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Cooling times (tcool) for TNG (dotted lines) and the SC SAM (dashed squares). The left and middle panels show the time evolution of tcool for cold-mode (rcool > rvir) and hot-mode (rcool < rvir) halos, respectively, at z = 1, 2, 6. The solid lines represent the dynamical time at the given redshift. In TNG, tcool generally remains above the dynamical time for both modes, highlighting the limitations of the… view at source ↗
Figure 12
Figure 12. Figure 12: Spatial distribution of matched halos between TNG100 and the TNG SAM at z = 0, plotted in physical space (x vs. y position). All TNG100 halos with 10.6 < log Mhalo < 12 are shown in white. The map is divided into seven sectors corresponding to a specific galaxy property: hot gas mass, cold gas mass, stellar mass, star formation rate, and metallicities of hot gas, cold gas, and stars. Each matched galaxy i… view at source ↗
Figure 13
Figure 13. Figure 13: Comparison of Mhot, Mcold, Mstarand SFR between the fiducial TNG100 model implemented in a 36.9 3 comoving Mpc3 volume (black dotted lines) and an otherwise identical variant that excludes black holes (green dashed crosses). At lower halo masses (log Mhalo< 11.2), the two models generally agree within ±30%. At higher halo masses (log Mhalo≳ 11.2), galaxy-scale properties differ substantially by up to a fa… view at source ↗
Figure 14
Figure 14. Figure 14: Comparison of the Santa Cruz SAM used in this work (dashed squares) to the Santa Cruz SAM presented in Gabrielpillai et al. 2022 (dashed circles) for Mhot. The original SC SAM’s cooling model depleted the CGM by up to ∼ 120% relative to the updated model presented here. While the revised cooling prescription produces a substantially less depleted hot halo, the updated SC SAM still underpredicts Mhot relat… view at source ↗
Figure 15
Figure 15. Figure 15: Extension of [PITH_FULL_IMAGE:figures/full_fig_p036_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: Extension of [PITH_FULL_IMAGE:figures/full_fig_p037_16.png] view at source ↗
Figure 17
Figure 17. Figure 17: Galaxy-scale properties and baryon flow rates for the TNG SAM calibrated using only ∼ 100 randomly selected galaxies per redshift. The figure follows the same layout, quantities, and redshift color-coding as [PITH_FULL_IMAGE:figures/full_fig_p038_17.png] view at source ↗
Figure 18
Figure 18. Figure 18: Halo-scale quantities and baryon flow rates for the TNG SAM calibrated using only ∼ 100 randomly selected galaxies per redshift, shown using the same layout and redshift color scheme as [PITH_FULL_IMAGE:figures/full_fig_p039_18.png] view at source ↗
read the original abstract

All cosmological models of galaxy formation must navigate the trade-off between physical accuracy and computational efficiency. Hydrodynamical simulations provide spatially resolved predictions for the co-evolution of dark matter, gas, stars, and black holes, but rely on phenomenological subgrid models for small-scale processes (e.g., star formation). Semi-analytic models (SAMs), by contrast, gain efficiency through simplified, analytic treatments of the same processes, at the cost of reduced predictive scope. In this work, we leverage the strengths of the Santa Cruz SAM and the IllustrisTNG hydrodynamical simulation to develop the TNG SAM. Calibrated to reproduce baryon cycling in stellar feedback-dominated TNG galaxies ($\sim 10^{10}M_\odot < M_{200} < 10^{12}M_\odot$), the TNG SAM introduces several key updates to the Santa Cruz framework regarding: 1) halo gas (re-)accretion efficiency, 2) a cooling model that moves beyond the traditional cold/hot mode dichotomy, 3) explicit treatment of both galactic- and halo-scale outflows, 4) star formation efficiency, and 5) the circulation of metals between galaxies and their surroundings. These changes enable the TNG SAM to reproduce TNG's flow of gas and metals from the scale of the galaxy to the halo, as well as global galaxy (e.g., stellar mass) and halo (e.g. hot halo gas mass) properties within $\lesssim 30\%$ accuracy out to $z=6$. This work demonstrates that, with appropriate calibration, SAMs can capture the complex physics of galaxy formation modeled in hydrodynamical simulations while providing a flexible framework for studying galaxy evolution across the large cosmological volumes targeted by future observational surveys.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 0 minor

Summary. The manuscript introduces the TNG SAM, an updated version of the Santa Cruz semi-analytic model incorporating five changes (halo gas re-accretion efficiency, a cooling model beyond the cold/hot dichotomy, explicit galactic- and halo-scale outflows, star formation efficiency, and metal circulation parameters) that are calibrated to reproduce baryon cycling and global properties (stellar mass, hot halo gas, metals) from the IllustrisTNG hydrodynamical simulation for stellar-feedback-dominated galaxies in the halo mass range ~10^10 < M_200 < 10^12 M_⊙, achieving agreement within ≲30% out to z=6.

Significance. If the calibrated parameters capture essential baryon cycling physics rather than fitting the narrow calibration domain, the result would be significant for enabling efficient modeling of galaxy evolution over the large cosmological volumes needed for future surveys while retaining key aspects of hydrodynamical complexity; however, the presented evidence consists solely of post-calibration agreement without independent validation.

major comments (2)
  1. [Abstract] Abstract: the reproduction of TNG gas flows, metal circulation, stellar mass, and hot halo gas mass to ≲30% is achieved by explicit calibration of the five model updates to TNG data in the stated mass range; the manuscript provides no independent validation tests outside ~10^10–10^12 M_⊙ or in AGN-feedback regimes, which is load-bearing for the claim that the updates enable accuracy across redshifts and properties.
  2. [Abstract] Abstract: no details are supplied on the procedure used to choose or constrain the five free parameters (halo gas re-accretion efficiency, cooling model parameters, outflow parameters, star formation efficiency, metal circulation parameters), making it impossible to determine whether the reported match reflects captured physics or is by construction within the fitted parameter space.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive report and for highlighting the need for greater clarity in the abstract regarding the calibration domain and parameter selection. We agree that revisions are warranted to avoid any implication of independent validation or unspecified fitting procedures. We respond to each major comment below and will update the abstract and, where appropriate, the methods section in the revised manuscript.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the reproduction of TNG gas flows, metal circulation, stellar mass, and hot halo gas mass to ≲30% is achieved by explicit calibration of the five model updates to TNG data in the stated mass range; the manuscript provides no independent validation tests outside ~10^10–10^12 M_⊙ or in AGN-feedback regimes, which is load-bearing for the claim that the updates enable accuracy across redshifts and properties.

    Authors: We agree that the reported agreement is the direct result of calibration to TNG within 10^10 < M_200 < 10^12 M_⊙ for stellar-feedback-dominated galaxies and that no independent validation outside this range or in AGN-feedback regimes is presented. The abstract already qualifies the results as calibrated, but we will revise it to state explicitly that the ≲30% accuracy holds within the calibrated domain and redshift range, without claiming broader applicability. This addresses the concern that the claim is load-bearing; the revised wording will limit the scope to the stellar-feedback regime where the updates were tuned. revision: yes

  2. Referee: [Abstract] Abstract: no details are supplied on the procedure used to choose or constrain the five free parameters (halo gas re-accretion efficiency, cooling model parameters, outflow parameters, star formation efficiency, metal circulation parameters), making it impossible to determine whether the reported match reflects captured physics or is by construction within the fitted parameter space.

    Authors: The full manuscript includes a methods section that describes the iterative calibration process used to constrain the five parameters against TNG baryon-cycle diagnostics. To ensure the abstract is self-contained, we will add a brief clause summarizing that the parameters were adjusted via targeted matching to TNG gas and metal flow rates, star-formation efficiencies, and outflow loadings within the stated mass range. This will clarify that the procedure is not arbitrary but is documented in the paper, while still acknowledging that the match is by design within the calibration space. revision: yes

Circularity Check

1 steps flagged

TNG SAM reproduction of TNG properties achieved by explicit calibration to TNG data

specific steps
  1. fitted input called prediction [Abstract]
    "Calibrated to reproduce baryon cycling in stellar feedback-dominated TNG galaxies (∼10^{10}M_⊙<M_{200}<10^{12}M_⊙), the TNG SAM introduces several key updates to the Santa Cruz framework regarding: 1) halo gas (re-)accretion efficiency, 2) a cooling model that moves beyond the traditional cold/hot mode dichotomy, 3) explicit treatment of both galactic- and halo-scale outflows, 4) star formation efficiency, and 5) the circulation of metals between galaxies and their surroundings. These changes enable the TNG SAM to reproduce TNG's flow of gas and metals ... within ≲30% accuracy out to z=6."

    The five updates are introduced and then stated to enable reproduction of the same TNG quantities to which the model was calibrated. The reported agreement is therefore enforced by the calibration step rather than emerging as a separate result.

full rationale

The paper's core claim is that the updated Santa Cruz SAM reproduces TNG baryon cycling, gas/metal flows, stellar masses, and halo gas masses to ≲30% out to z=6. This match is obtained after the model is calibrated to TNG galaxies in the stellar-feedback-dominated window 10^10 < M_200 < 10^12 M_⊙. The reproduction therefore reduces directly to the fitting procedure within the calibrated domain rather than constituting an independent derivation or prediction.

Axiom & Free-Parameter Ledger

5 free parameters · 2 axioms · 0 invented entities

The model depends on multiple calibration parameters for the five listed updates plus standard assumptions of hierarchical merging and analytic baryon cycling; no new entities are postulated.

free parameters (5)
  • halo gas re-accretion efficiency
    Calibrated to match TNG baryon cycling in the target mass range
  • cooling model parameters
    Updated beyond traditional cold/hot mode split
  • galactic- and halo-scale outflow parameters
    Explicit treatment calibrated to TNG
  • star formation efficiency
    Calibrated to TNG galaxies
  • metal circulation parameters
    Calibrated to reproduce TNG metal flows
axioms (2)
  • standard math Hierarchical merging and structure formation in ΛCDM cosmology
    Background framework for all SAMs
  • domain assumption Baryon cycling can be captured by analytic prescriptions with five targeted updates
    Core modeling choice stated in abstract

pith-pipeline@v0.9.1-grok · 5895 in / 1526 out tokens · 53932 ms · 2026-06-26T23:38:32.673470+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

132 extracted references · 131 canonical work pages · 18 internal anchors

  1. [1]

    , archivePrefix = "arXiv", eprint =

    A semi-analytic model for the co-evolution of galaxies, black holes and active galactic nuclei , volume =. MNRAS , author =. 2008 , keywords =. doi:10.1111/j.1365-2966.2008.13805.x , abstract =

    work page doi:10.1111/j.1365-2966.2008.13805.x 2008

  2. [2]

    2018, MNRAS, 475, 676, doi: 10.1093/mnras/stx3304

    First results from the. MNRAS , author =. 2018 , pages =. doi:10.1093/mnras/stx3304 , abstract =

    work page doi:10.1093/mnras/stx3304 2018

  3. [3]

    , archivePrefix = "arXiv", eprint =

    E pur si muove:. MNRAS , author =. 2010 , pages =. doi:10.1111/j.1365-2966.2009.15715.x , abstract =

    work page doi:10.1111/j.1365-2966.2009.15715.x 2010

  4. [4]

    and Leroy, A

    Bigiel, F. and Leroy, A. and Walter, F. and Brinks, E. and de Blok, W. J. G. and Madore, B. and Thornley, M. D. , month =. The. 2008 , comment =. doi:10.1088/0004-6256/136/6/2846 , journal=

    work page doi:10.1088/0004-6256/136/6/2846 2008

  5. [5]

    Benson, A. J. and Bower, R. G. and Frenk, C. S. and Lacey, C. G. and Baugh, C. M. and Cole, S. , month =. What. 2003 , comment =. doi:10.1086/379160 , journal=

    work page doi:10.1086/379160 2003

  6. [6]

    Kennicutt, Jr., R. C. , month =. The. 1998 , comment =. doi:10.1086/305588 , journal=

    work page internal anchor Pith review doi:10.1086/305588 1998

  7. [7]

    Sutherland, R. S. and Dopita, M. A. , month =. Cooling functions for low-density astrophysical plasmas , volume =. 1993 , keywords =. doi:10.1086/191823 , journal=

    work page doi:10.1086/191823 1993

  8. [8]

    Bower, R. G. and Benson, A. J. and Malbon, R. and Helly, J. C. and Frenk, C. S. and Baugh, C. M. and Cole, S. and Lacey, C. G. , month =. Breaking the hierarchy of galaxy formation , volume =. 2006 , comment =. doi:10.1111/j.1365-2966.2006.10519.x , journal=

    work page doi:10.1111/j.1365-2966.2006.10519.x 2006

  9. [9]

    Croton, D. J. and Springel, V. and White, S. D. M. and De Lucia, G. and Frenk, C. S. and Gao, L. and Jenkins, A. and Kauffmann, G. and Navarro, J. F. and Yoshida, N. , month =. The many lives of active galactic nuclei: cooling flows, black holes and the luminosities and colours of galaxies , volume =. 2006 , comment =. doi:10.1111/j.1365-2966.2005.09675.x...

    work page doi:10.1111/j.1365-2966.2005.09675.x 2006

  10. [10]

    , keywords =

    Characterizing mass, momentum, energy, and metal outflow rates of multiphase galactic winds in the. MNRAS , author =. 2021 , keywords =. doi:10.1093/mnras/stab2714 , abstract =

    work page doi:10.1093/mnras/stab2714 2021

  11. [11]

    and Angles-Alcazar, Daniel and Hayward, Christopher C

    Pandya, Viraj and Somerville, Rachel S. and Angles-Alcazar, Daniel and Hayward, Christopher C. and Bryan, Greg L. and Fielding, Drummond B. and Forbes, John C. and Burkhart, Blakesley and Genel, Shy and Hernquist, Lars and Kim, Chang-Goo and Tonnesen, Stephanie and Starkenburg, Tjitske , month =. First. ApJ , publisher =. 2020 , keywords =. doi:10.3847/15...

    work page doi:10.3847/1538-4357/abc3c1 2020

  12. [12]

    MNRAS , author =

    The evolution of the mass-metallicity relation and its scatter in. MNRAS , author =. 2019 , file =. doi:10.1093/mnras/stz243 , abstract =

    work page doi:10.1093/mnras/stz243 2019

  13. [13]

    MNRAS , author =

    Atomic and molecular gas in. MNRAS , author =. 2019 , comment =. doi:10.1093/mnras/stz1323 , abstract =

    work page doi:10.1093/mnras/stz1323 2019

  14. [14]

    2018a, MNRAS, 473, 4077, doi: 10.1093/mnras/stx2656

    Simulating. MNRAS , author =. 2018 , comment =. doi:10.1093/mnras/stx2656 , abstract =

    work page internal anchor Pith review doi:10.1093/mnras/stx2656 2018

  15. [15]

    and Davé, Romeel , year=

    Physical. ARA&A , author =. 2015 , comment =. doi:10.1146/annurev-astro-082812-140951 , abstract =

    work page internal anchor Pith review doi:10.1146/annurev-astro-082812-140951 2015

  16. [16]

    MNRAS , author =

    Constraining the galaxy-halo connection over the last 13.3. MNRAS , author =. 2017 , comment =. doi:10.1093/mnras/stx1172 , abstract =

    work page doi:10.1093/mnras/stx1172 2017

  17. [17]

    , archivePrefix = "arXiv", eprint =

    Robitaille, Thomas P. and Tollerud, Erik J. and Greenfield, Perry and Droettboom, Michael and Bray, Erik and Aldcroft, Tom and Davis, Matt and Ginsburg, Adam and Price-Whelan, Adrian M. and Kerzendorf, Wolfgang E. and Conley, Alexander and Crighton, Neil and Barbary, Kyle and Muna, Demitri and Ferguson, Henry and Grollier, Frederic and Parikh, Madhura M. ...

    work page doi:10.1051/0004-6361/201322068 2013

  18. [18]

    MNRAS , author =

    Galactic outflow rates in the. MNRAS , author =. 2020 , pages =. doi:10.1093/mnras/staa938 , abstract =

    work page doi:10.1093/mnras/staa938 2020

  19. [19]

    MNRAS , author =

    The impact of stellar and. MNRAS , author =. 2020 , pages =. doi:10.1093/mnras/staa2359 , abstract =

    work page doi:10.1093/mnras/staa2359 2020

  20. [20]

    Matching the observed evolution of star formation rates, colours and stellar masses

    Galaxy formation in the. MNRAS , author =. 2015 , pages =. doi:10.1093/mnras/stv705 , abstract =

    work page doi:10.1093/mnras/stv705 2015

  21. [21]

    E., et al

    Virtanen, Pauli and Gommers, Ralf and Oliphant, Travis E. and Haberland, Matt and Reddy, Tyler and Cournapeau, David and Burovski, Evgeni and Peterson, Pearu and Weckesser, Warren and Bright, Jonathan and van der Walt, Stefan J. and Brett, Matthew and Wilson, Joshua and Millman, K. Jarrod and Mayorov, Nikolay and Nelson, Andrew R. J. and Jones, Eric and K...

    work page doi:10.1038/s41592-019-0686-2 2020

  22. [22]

    C., & Varoquaux , G

    The. Computing in Science & Engineering , author =. 2011 , comment =. doi:10.1109/MCSE.2011.37 , abstract =

    work page doi:10.1109/mcse.2011.37 2011

  23. [23]

    Caswell, Thomas A. and Lee, Antony and Droettboom, Michael and Andrade, Elliott Sales de and Hoffmann, Tim and Klymak, Jody and Hunter, John and Firing, Eric and Stansby, David and Varoquaux, Nelle and Nielsen, Jens Hedegaard and Root, Benjamin and May, Ryan and Elson, Phil and Seppanen, Jouni K. and Dale, Darren and Lee, Jae-Joon and McDougall, Damon and...

    work page doi:10.5281/zenodo.6982547 2022

  24. [24]

    , Title =

    Perez, Fernando and Granger, Brian E. , month =. Computing in Science & Engineering , publisher =. 2007 , pages =. doi:10.1109/MCSE.2007.53 , abstract =

    work page doi:10.1109/mcse.2007.53 2007

  25. [25]

    Simulating galaxy formation with black hole driven thermal and kinetic feedback

    Simulating galaxy formation with black hole driven thermal and kinetic feedback , volume =. MNRAS , author =. 2017 , pages =. doi:10.1093/mnras/stw2944 , abstract =

    work page internal anchor Pith review doi:10.1093/mnras/stw2944 2017

  26. [26]

    2018b, MNRAS, 475, 648, doi: 10.1093/mnras/stx3112 Planck Collaboration, Ade, P

    First results from the. MNRAS , author =. 2018 , pages =. doi:10.1093/mnras/stx3112 , abstract =

    work page internal anchor Pith review doi:10.1093/mnras/stx3112 2018

  27. [27]

    2019, MNRAS, 490, 3196, doi: 10.1093/mnras/stz2338

    First results from the. MNRAS , author =. 2019 , pages =. doi:10.1093/mnras/stz2338 , abstract =

    work page doi:10.1093/mnras/stz2338 2019

  28. [28]

    2016 , pages =

    A&A , author =. 2016 , pages =. doi:10.1051/0004-6361/201525830 , language =

    work page doi:10.1051/0004-6361/201525830 2016

  29. [29]

    2018, MNRAS, 475, 624, doi: 10.1093/mnras/stx3040

    First results from the. MNRAS , author =. 2018 , pages =. doi:10.1093/mnras/stx3040 , abstract =

    work page internal anchor Pith review doi:10.1093/mnras/stx3040 2018

  30. [30]

    2019, MNRAS, 490, 3234, doi: 10.1093/mnras/stz2306

    First results from the. MNRAS , author =. 2019 , pages =. doi:10.1093/mnras/stz2306 , abstract =

    work page internal anchor Pith review doi:10.1093/mnras/stz2306 2019

  31. [31]

    Anderson, L. D. and Bania, T. M. and Balser, Dana S. and Cunningham, V. and Wenger, T. V. and Johnstone, B. M. and Armentrout, W. P. , month =. ApJS , publisher =. 2014 , pages =. doi:10.1088/0067-0049/212/1/1 , abstract =

    work page doi:10.1088/0067-0049/212/1/1 2014

  32. [32]

    , year = 1999, volume =

    Semi-analytic modelling of galaxy formation: the local. MNRAS , author =. 1999 , pages =. doi:10.1046/j.1365-8711.1999.03032.x , abstract =

    work page doi:10.1046/j.1365-8711.1999.03032.x 1999

  33. [33]

    Sanchez, S. F. and Kennicutt, R. C. and Paz, A. Gil de and Ven, G. van de and Vilchez, J. M. and Wisotzki, L. and Walcher, C. J. and Mast, D. and Aguerri, J. a. L. and Albiol-Perez, S. and Alonso-Herrero, A. and Alves, J. and Bakos, J. and Bartakova, T. and Bland-Hawthorn, J. and Boselli, A. and Bomans, D. J. and Castillo-Morales, A. and Cortijo-Ferrero, ...

    work page doi:10.1051/0004-6361/201117353 2012

  34. [34]

    MNRAS , author =

    Galaxy formation in the. MNRAS , author =. 2022 , pages =. doi:10.1093/mnras/stac2297 , abstract =

    work page doi:10.1093/mnras/stac2297 2022

  35. [35]

    MNRAS , author =

    The relationship between black hole mass and galaxy properties: examining the black hole feedback model in. MNRAS , author =. 2020 , pages =. doi:10.1093/mnras/staa374 , abstract =

    work page doi:10.1093/mnras/staa374 2020

  36. [36]

    MNRAS , author =

    Star formation in semi-analytic galaxy formation models with multiphase gas , volume =. MNRAS , author =. 2015 , pages =. doi:10.1093/mnras/stv1877 , abstract =

    work page doi:10.1093/mnras/stv1877 2015

  37. [37]

    , keywords =

    A comparison of semi-analytic and smoothed particle hydrodynamics galaxy formation , volume =. MNRAS , author =. 2001 , pages =. doi:10.1046/j.1365-8711.2001.03966.x , abstract =

    work page doi:10.1046/j.1365-8711.2001.03966.x 2001

  38. [38]

    , eprint =

    A comparison of gas dynamics in smooth particle hydrodynamics and semi-analytic models of galaxy formation , volume =. MNRAS , author =. 2003 , pages =. doi:10.1046/j.1365-8711.2003.06152.x , abstract =

    work page doi:10.1046/j.1365-8711.2003.06152.x 2003

  39. [39]

    , archivePrefix = "arXiv", eprint =

    Analytic and numerical realizations of a disc galaxy , volume =. MNRAS , author =. 2010 , pages =. doi:10.1111/j.1365-2966.2010.16944.x , abstract =

    work page doi:10.1111/j.1365-2966.2010.16944.x 2010

  40. [40]

    , archivePrefix = "arXiv", eprint =

    Galaxy formation in semi-analytic models and cosmological hydrodynamic zoom simulations , volume =. MNRAS , author =. 2012 , pages =. doi:10.1111/j.1365-2966.2011.19961.x , abstract =

    work page doi:10.1111/j.1365-2966.2011.19961.x 2012

  41. [41]

    MNRAS , author =

    Galaxies in the. MNRAS , author =. 2016 , pages =. doi:10.1093/mnras/stw1525 , abstract =

    work page doi:10.1093/mnras/stw1525 2016

  42. [42]

    2013, MNRAS, 436, 3031, doi: 10.1093/mnras/stt1789

    A model for cosmological simulations of galaxy formation physics , volume =. MNRAS , author =. 2013 , pages =. doi:10.1093/mnras/stt1789 , abstract =

    work page internal anchor Pith review doi:10.1093/mnras/stt1789 2013

  43. [43]

    , keywords =

    Gas cooling in simulations of the formation of the galaxy population , volume =. MNRAS , author =. 2002 , pages =. doi:10.1046/j.1365-8711.2002.05661.x , abstract =

    work page doi:10.1046/j.1365-8711.2002.05661.x 2002

  44. [44]

    , archivePrefix = "arXiv", eprint =

    Magnetohydrodynamics on an unstructured moving grid , volume =. MNRAS , author =. 2011 , pages =. doi:10.1111/j.1365-2966.2011.19591.x , abstract =

    work page doi:10.1111/j.1365-2966.2011.19591.x 2011

  45. [45]

    MNRAS , author =

    Simulations of magnetic fields in isolated disc galaxies , volume =. MNRAS , author =. 2013 , pages =. doi:10.1093/mnras/stt428 , abstract =

    work page doi:10.1093/mnras/stt428 2013

  46. [46]

    FIRE-2 Simulations: Physics versus Numerics in Galaxy Formation

    MNRAS , author =. 2018 , pages =. doi:10.1093/mnras/sty1690 , abstract =

    work page internal anchor Pith review doi:10.1093/mnras/sty1690 2018

  47. [47]

    2014, MNRAS, 438, 1985, doi: 10.1093/mnras/stt2295

    A model for cosmological simulations of galaxy formation physics: multi-epoch validation , volume =. MNRAS , author =. 2014 , pages =. doi:10.1093/mnras/stt2295 , abstract =

    work page doi:10.1093/mnras/stt2295 2014

  48. [48]

    , keywords =

    Galaxy properties from the ultraviolet to the far-infrared: L cold dark matter models confront observations , volume =. MNRAS , author =. 2012 , pages =. doi:10.1111/j.1365-2966.2012.20490.x , abstract =

    work page doi:10.1111/j.1365-2966.2012.20490.x 2012

  49. [49]

    MNRAS , author =

    Understanding the structural scaling relations of early-type galaxies , volume =. MNRAS , author =. 2014 , pages =. doi:10.1093/mnras/stu1434 , abstract =

    work page doi:10.1093/mnras/stu1434 2014

  50. [50]

    MNRAS , author =

    Semi-analytic forecasts for. MNRAS , author =. 2023 , pages =. doi:10.1093/mnras/stac3595 , abstract =

    work page doi:10.1093/mnras/stac3595 2023

  51. [51]

    MNRAS , author =

    Evolution of the atomic and molecular gas content of galaxies , volume =. MNRAS , author =. 2014 , pages =. doi:10.1093/mnras/stu991 , abstract =

    work page doi:10.1093/mnras/stu991 2014

  52. [52]

    Collaboration, The Astropy and Price-Whelan, A. M. and Sipocz, B. M. and Gunther, H. M. and Lim, P. L. and Crawford, S. M. and Conseil, S. and Shupe, D. L. and Craig, M. W. and Dencheva, N. and Ginsburg, A. and VanderPlas, J. T. and Bradley, L. D. and Perez-Suarez, D. and Val-Borro, M. de and Contributors), (Primary Paper and Aldcroft, T. L. and Cruz, K. ...

    work page doi:10.3847/1538-3881/aabc4f 2018

  53. [53]

    M., Lim, P

    Collaboration, The Astropy and Price-Whelan, Adrian M. and Lim, Pey Lian and Earl, Nicholas and Starkman, Nathaniel and Bradley, Larry and Shupe, David L. and Patil, Aarya A. and Corrales, Lia and Brasseur, C. E. and Nothe, Maximilian and Donath, Axel and Tollerud, Erik and Morris, Brett M. and Ginsburg, Adam and Vaher, Eero and Weaver, Benjamin A. and To...

    work page internal anchor Pith review doi:10.3847/1538-4357/ac7c74 2022

  54. [54]

    The Rockstar Phase-Space Temporal Halo Finder and the Velocity Offsets of Cluster Cores

    Behroozi, Peter S. and Wechsler, Risa H. and Wu, Hao-Yi , month =. ApJ , publisher =. 2012 , pages =. doi:10.1088/0004-637X/762/2/109 , abstract =

    work page internal anchor Pith review doi:10.1088/0004-637x/762/2/109 2012

  55. [55]

    , keywords =

    The evolution of large-scale structure in a universe dominated by cold dark matter , volume =. ApJ , author =. 1985 , pages =. doi:10.1086/163168 , abstract =

    work page doi:10.1086/163168 1985

  56. [56]

    , archivePrefix = "arXiv", eprint =

    Mass loss of galaxies due to an ultraviolet background , volume =. MNRAS , author =. 2008 , pages =. doi:10.1111/j.1365-2966.2008.13830.x , abstract =

    work page doi:10.1111/j.1365-2966.2008.13830.x 2008

  57. [57]

    and Barden, Marco and Rix, Hans-Walter and Bell, Eric F

    Somerville, Rachel S. and Barden, Marco and Rix, Hans-Walter and Bell, Eric F. and Beckwith, Steven V. W. and Borch, Andrea and Caldwell, John A. R. and Haussler, Boris and Heymans, Catherine and Jahnke, Knud and Jogee, Shardha and McIntosh, Daniel H. and Meisenheimer, Klaus and Peng, Chien Y. and Sanchez, Sebastian F. and Wisotzki, Lutz and Wolf, Christi...

    work page doi:10.1086/523661 2008

  58. [58]

    , keywords =

    A general model for the. MNRAS , author =. 2012 , pages =. doi:10.1111/j.1365-2966.2012.20536.x , abstract =

    work page doi:10.1111/j.1365-2966.2012.20536.x 2012

  59. [59]

    and Kravtsov, Andrey V

    Gnedin, Nickolay Y. and Kravtsov, Andrey V. , month =. ApJ , publisher =. 2011 , pages =. doi:10.1088/0004-637X/728/2/88 , abstract =

    work page doi:10.1088/0004-637x/728/2/88 2011

  60. [60]

    , keywords =

    Galaxy formation through hierarchical clustering , volume =. ApJ , author =. 1991 , pages =. doi:10.1086/170483 , abstract =

    work page doi:10.1086/170483 1991

  61. [61]

    and Frenk, Carlos S

    The. ApJ , author =. 1996 , comment =. doi:10.1086/177173 , abstract =

    work page doi:10.1086/177173 1996

  62. [62]

    , keywords =

    Pandya, Viraj and Fielding, Drummond B. and Bryan, Greg L. and Carr, Christopher and Somerville, Rachel S. and Stern, Jonathan and Faucher-Giguere, Claude-Andre and Hafen, Zachary and Angles-Alcazar, Daniel and Forbes, John C. , month =. A. ApJ , publisher =. 2023 , pages =. doi:10.3847/1538-4357/acf3ea , language =

    work page doi:10.3847/1538-4357/acf3ea 2023

  63. [63]

    MNRAS , author =

    Comparing galaxy formation in semi-analytic models and hydrodynamical simulations , volume =. MNRAS , author =. 2018 , pages =. doi:10.1093/mnras/stx2770 , abstract =

    work page doi:10.1093/mnras/stx2770 2018

  64. [64]

    , eprint =

    Cosmological smoothed particle hydrodynamics simulations: a hybrid multiphase model for star formation , volume =. MNRAS , author =. 2003 , pages =. doi:10.1046/j.1365-8711.2003.06206.x , abstract =

    work page doi:10.1046/j.1365-8711.2003.06206.x 2003

  65. [65]

    2019, MNRAS, 485, 4817, doi: 10.1093/mnras/stz712

    The star formation activity of. MNRAS , author =. 2019 , pages =. doi:10.1093/mnras/stz712 , abstract =

    work page doi:10.1093/mnras/stz712 2019

  66. [66]

    and O'Shea, Brian W

    Cote, Benoit and Silvia, Devin W. and O'Shea, Brian W. and Smith, Britton and Wise, John H. , month =. Validating. ApJ , publisher =. 2018 , pages =. doi:10.3847/1538-4357/aabe8f , abstract =

    work page doi:10.3847/1538-4357/aabe8f 2018

  67. [67]

    , keywords =

    Hydrodynamical simulations and semi-analytic models of galaxy formation: two sides of the same coin , volume =. MNRAS , author =. 2012 , pages =. doi:10.1111/j.1365-2966.2012.20584.x , abstract =

    work page doi:10.1111/j.1365-2966.2012.20584.x 2012

  68. [68]

    , archivePrefix = "arXiv", eprint =

    Gas cooling in semi-analytic models and smoothed particle hydrodynamics simulations: are results consistent? , volume =. MNRAS , author =. 2010 , pages =. doi:10.1111/j.1365-2966.2010.16737.x , abstract =

    work page doi:10.1111/j.1365-2966.2010.16737.x 2010

  69. [69]

    MNRAS , author =

    A semi-analytic model comparison: testing cooling models against hydrodynamical simulations , volume =. MNRAS , author =. 2014 , pages =. doi:10.1093/mnras/stu655 , abstract =

    work page doi:10.1093/mnras/stu655 2014

  70. [70]

    and Turk, Matthew J

    Wise, John H. and Turk, Matthew J. and Norman, Michael L. and Abel, Tom , month =. ApJ , publisher =. 2011 , pages =. doi:10.1088/0004-637X/745/1/50 , abstract =

    work page doi:10.1088/0004-637x/745/1/50 2011

  71. [71]

    Monthly Notices of the Royal Astronomical Society , volume =

    The size evolution of star-forming and quenched galaxies in the. MNRAS , author =. 2018 , pages =. doi:10.1093/mnras/stx3078 , abstract =

    work page doi:10.1093/mnras/stx3078 2018

  72. [72]

    Pandya, Viraj , year =. Semi-

  73. [73]

    , archivePrefix = "arXiv", eprint =

    From dwarf spheroidals to. MNRAS , author =. 2011 , pages =. doi:10.1111/j.1365-2966.2010.18114.x , abstract =

    work page doi:10.1111/j.1365-2966.2010.18114.x 2011

  74. [74]

    , archivePrefix = "arXiv", eprint =

    Constraints on star formation driven galaxy winds from the mass-metallicity relation at z= 0 , volume =. MNRAS , author =. 2011 , pages =. doi:10.1111/j.1365-2966.2011.19456.x , abstract =

    work page doi:10.1111/j.1365-2966.2011.19456.x 2011

  75. [75]

    Diemer, Benedikt and Stevens, Adam R. H. and Forbes, John C. and Marinacci, Federico and Hernquist, Lars and Lagos, Claudia del P. and Sternberg, Amiel and Pillepich, Annalisa and Nelson, Dylan and Popping, Gergo and Villaescusa-Navarro, Francisco and Torrey, Paul and Vogelsberger, Mark , month =. Modeling the. ApJS , publisher =. 2018 , pages =. doi:10.3...

    work page doi:10.3847/1538-4365/aae387 2018

  76. [76]

    and Fielding, Drummond B

    Carr, Christopher and Bryan, Greg L. and Fielding, Drummond B. and Pandya, Viraj and Somerville, Rachel S. , month =. Regulation of. ApJ , publisher =. 2023 , pages =. doi:10.3847/1538-4357/acc4c7 , abstract =

    work page doi:10.3847/1538-4357/acc4c7 2023

  77. [77]

    MNRAS , author =

    How gas flows shape the stellar-halo mass relation in the eagle simulation , volume =. MNRAS , author =. 2022 , pages =. doi:10.1093/mnras/stab3339 , abstract =

    work page doi:10.1093/mnras/stab3339 2022

  78. [78]

    , archivePrefix = "arXiv", eprint =

    The degeneracy of galaxy formation models , volume =. MNRAS , author =. 2010 , pages =. doi:10.1111/j.1365-2966.2010.16656.x , abstract =

    work page doi:10.1111/j.1365-2966.2010.16656.x 2010

  79. [79]

    2018, MNRAS, 480, 5113, doi: 10.1093/mnras/sty2206

    First results from the. MNRAS , author =. 2018 , pages =. doi:10.1093/mnras/sty2206 , abstract =

    work page internal anchor Pith review doi:10.1093/mnras/sty2206 2018

  80. [80]

    K., et al

    The massive end of the luminosity and stellar mass functions: dependence on the fit to the light profile , volume =. MNRAS , author =. 2013 , pages =. doi:10.1093/mnras/stt1607 , abstract =

    work page internal anchor Pith review doi:10.1093/mnras/stt1607 2013

Showing first 80 references.